Mass transfer in interacting binaries: The Oil on Water SPH method
Binary stellar systems, contain two stars orbiting their common centre of
mass under the effect of their mutual gravitational attraction. Binaries are
very common in nature: about two thirds of Sun-like stars are found in binary
systems. Many interesting astronomical objects are formed from mass-transfer
binaries, including cataclysmic variables, X-ray binaries and type IA
supernovae.
For binaries undergoing equilibrium mass transfer in circular binaries the
theory of mass transfer is well-established. If a star overfills its
Roche Lobe, the potential surface that connects both stars, then
matter will flow from one star to the other. However, many systems undergo
non-equillibrium mass transfer. Eccentric binaries come in and out of
contact on each orbit, transferring mass only during the closest approach.
Many stars first transfer mass during the red giant phase, when they are
large cool stars up to 1000 times the size of the Sun. This mass transfer is
unstable, and leads to a common envelope of low density gas surrounding both
stars. This process in inherently non-equilibrium and cannot be followed
within the Roche formalism.
To follow non-equilibrium mass transfer in binary systems we have developed
a new extension to SPH, a particle-based Lagrangian hydrodynamic technique.
In order to model typical mass transfer rates where as little as one part
in 1012 of the star's mass is transferred during each closest
approach we have constructed a two-phase system. A layer of light oil
particles floats on top of the dense water particles that dominate
the mass of the star. The details of the model are described by Church et al. (2009).
IMAGE 3:
A cartoon showing the Oil on Water operation.
Using the Oil on Water formalism we have modelled the evolution of eccentric
binaries containing a low-mass main-sequence star and a white dwarf. We use
about 30 000 particles in the stellar atmosphere in order to be able to
resolve layers of different densities. The video below shows the motion of
the oil particles in a slice through the centre of the orbit; the water
particles are omitted for clarity. The eccentricity in this simulation
is e=0.2. We follow for several orbits to show that the mass transfer
is stable and well-defined. An advantage of our method is that the oil
particles obey the full equations of SPH; the formation of a accretion disc
can be clearly seen in the video.
For more details, see the our paper on the topic
(Church et al. 2009, published in MNRAS), or email Ross Church and Melvyn B. Davies.